An Example of Blazar Blazar An Example of Multiwavelength - - PowerPoint PPT Presentation

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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An Example of An Example of Blazar Blazar Multiwavelength Multiwavelength Activities Activities as Prelude of the New as Prelude of the New Gamma Gamma-

• ray Era

ray Era

Stefano Ciprini Stefano Ciprini

I.N.F.N. Perugia & University of Perugia I.N.F.N. Perugia & University of Perugia

5th Science AGILE Workshop

AGILE’s First Year

• f Gamma-ray

Astrophysics

ESRIN, Frascati, Roma, 12-13 June, 2008

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

stefano.ciprini@pg.infn.it

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Summary Summary

Spectroscopy Polarization Variability Flux Monitoring Multiwaveband campaigns

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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ESO Very Large Telescope ESO Very Large Telescope high S/N spectroscopy of high S/N spectroscopy of blazars blazars

Quasi-featureless spectra of BL Lac objects hinders the determination of their redshifts. Anyway knowledge of blazars' distance is important to constraint their physics, their intrinsic bolometric emission power, to select the best gamma-ray blazar-probes for the study

• f the cosmic EBL, to have a rather sure classification of an high-energy source, and

sometimes to have a right blazar identification between close optical pair/multiple counterparts that can be put in the same slit and observation. In this view a program at the ESO 8m VLT for high S/N optical spectroscopy of BL Lac

• bjects lacking a firm redshift estimate is ongoing:

3 VLT runs accepted in 2003 and 2004 (ESO P71, P72, P73), all with PI A. Treves. 3 VLT run accepted in 2006, 2008 and 2008-09 (ESO P77, P81, P82) all with PI: S. Ciprini.

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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ESO Very Large Telescope ESO Very Large Telescope high S/N spectroscopy of high S/N spectroscopy of blazars blazars

Why the VLT 8-meter (315 inch) “monster” telescopes ? The 4m-telescope class has achieved its limit regarding to BL Lac with quasi-featureless optical spectra High S/N and spectral resolution needed in reasonable integration observing times. VLT run 2006 (P77) results: 15 observed

• bjects, 12 confirmed as BL Lac objects, 1 a sub-

DLA system, 1 reclassified as FSRQs, 1 misclassified, for 4 BL Lac objects a new

• determination. For the remaining 8 BL Lacs we

give redshift lower limits based on the minimum detectable equivalent width of their featureless spectra (Sbarufatti et al. 2008, AJ, submitted).

Adapted by Sbarufatti et al. 2008, AJ, submitted.

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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ESO Very Large Telescope ESO Very Large Telescope high S/N spectroscopy of high S/N spectroscopy of blazars blazars

Example of faint source-intrinsic lines detected: emission lines ([OIII], [NeIII], [MgII], [OII], H-beta, H-alpha, [NII], MgII); and absorption lines (CaII, MgI, G-band, and FeII, MgII in PKS 0823-223, a sub-damped Lyman-alpha absorber at z=0.91). Minimum Equivalent Width detected is between 0.09 and 1.84 A.

Adapted by Sbarufatti et al. 2008, AJ, submitted.

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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High degree (up to 3% to >30%) and variability of the optical polarization (OP) is one of the defining properties of blazars. OP observations are an important element in new blazar confirmation, when there is already a multiwaveband information about the candidates. High degree of OP is an evidence of strong non-thermal beamed radiation, the signature of a population of high-energy (HE) emitting particles (possibly producing also γ-rays), and provides information on source geometry and physics. Optical telescopes are biased to select optically bright blazars (i.e. possibly IBL, the best candidates to produce SSC GeV photons). The maximum level of information (polarization in particular) in the optical band is therefore desirable during AGILE/GLAST blazar observations. 1 run performed at the NOT (P31, PI S.Ciprini, but bad weather and only very few data

• btained). More proposals planned for the INAF-TNG.

Optical polarization snapshots of new Optical polarization snapshots of new blazar blazar candidates candidates

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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Aims: 1) to confirm or not their BL Lac or HPQ status, increasing the number of known blazars (useful for AGILE/GLAST source catalogs). 2) to have the first (or almost) measures of the optical polarization in such targets. Sample: possible, probable, new blazar candidates, and blazar with old/few/doubtful

• r no optical polarization measures. Mag(V)

range between 17-20 for 4-m telescopes. NOT-run results: 65% of the granted time lost due to bad weather. 6 objects could be confirmed as blazars (opt. pol. degree > 5%), but frame reanalysis needed. Future: other applications are though for 4-m telescopes (polarization snapshot surveys & dedicated 1-source polarization monitoring during MW campaigns) .

Optical polarization snapshots of new Optical polarization snapshots of new blazar blazar candidates candidates

An example of identification process for a EGRET gamma-ray

• source. Optical

polarization snapshots are an important ingredient in such process (Wallace et al. 2004). An example of intensive polarization monitoring of a bright blazar (PKS 2155-304) during the HESS campaign

• f 2004 (Ciprini

et al. 2006)

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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Example of Example of multiwavelength multiwavelength campaign campaign

XMM-Newton observations (4 osb., from 2005 to 2008) + coordinated WEBT intensive campaign (PI S Ciprini) And longer-term radio-optical monitoring + VLBA data.

XMM-Newton combined EPIC (pn, MOS1-MOS2) X-ray spectra

• f OJ 287, belonging to the 2 observations performed on Apr.12,

and Nov.3-4, 2005. Left panel: the Apr.12 spectrum can be described by a simple power-law + galactic absorption (Γ =1.63 ± 0.02). Right panel: the Nov.3-4 spectrum can be described by a broken power-law + galactic absorption (Γ1 = 2.65 -0.07/+0.12, and Γ2 = 1.79 ± 0.02) with break at 0.7 keV. Such X-ray data indicates different flux intensity, spectral continuum slopes, and emission components (From Ciprini et al. 2007, Ciprini et al. in prep.). The whole October 2004 - April 2006 optical light curve in R-band of OJ 287 obtained during our multiwavelength campaign. Data from more than 30

• bservatories. Intensive-observation data of about 1 week around the first

satellite pointing date, and from about 20 days around the second satellite pointing belongs to the international consortium WEBT. In particular an enduring outburst phase was observed at the beginning of the second season.

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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Long-term monitoring (OJ 287 2005-2008 Project and ENIGMA Campaign) begun in late 2004 (PM/CM: L. Takalo, A. Sillanpää ). VLBA radio structure/polarization observations in 5 bands: 6 times, 8h for the period 2005-2006 (more

• bs. planned in 2007-08) (PI: T. Savolainen).

VLBA and Global 3mm-VLBI radio-mm structure/polarization observations (as a calibrator, April 4 and 17, 2005, PI: I. Agudo). ESO VLT spectroscopic optical observations (4 epochs, PI: K. Nilsson). XMM-Newton X-ray observations: 2 pointings of about 40 ksec each in cycle AO-4 (April 12, and November 3-4, 2005, PI: S. Ciprini). A 3rd pointing performed in November 2006 (AO-5, PI: S. Ciprini). A 4th observation performed in April 2008 (AO-6, PI S. Ciprini). WEBT intensive ground-based MW campaign around the 2 XMM pointing epochs (CM: S. Ciprini) . ToO Effelsberg 100m radiotelescope flux/polarization observations on April 12 and Nov. 8-9-10 (ToO PI:

• L. Fuhrmann).

4 sessions of Global 3mm-VLBI observations in period Oct.2005-Apr.2007 (PI: E. Rastorgueva, K. Wiik). MAGIC gamma-ray Cherenkov telescope observations in January (10h) and November 2005 (>5h, this last in ToO mode, PI: E .Lindfors). Optical polarization monitoring at NOT (PI: K.Nilsson) and CalarAlto (2006-2008, PI: J. Heidt).

Some of the ongoing MW programs on OJ 287 (list probably not complete, sorry):

Example of Example of multiwavelength multiwavelength campaign campaign

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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Example of Example of multiwavelength multiwavelength campaign campaign

The OJ 287 campaign: some examples of the obtained near-IR & optical data galore!

The detailed (and best sampled) R-band magnitude light curve corresponding to the intensive coordinated campaign performed by the WEBT consortium, around the two XMM-Newton pointing dates. In the right panel, in particular, an enduring (more than 20 days), symmetrical, and time-structured (we 3 major rather symmetric wiggles), optical outburst is evident and confirmed by many observatories in the period October- November 2005. The brighter R band magnitude detected here was R = 13.2. (From Ciprini et al. 2007, Ciprini et al. in prep.).

UBVRIJHK multi-band optical and near-IR light curves of OJ 287 acquired during our long-term 2004-2006 campaign

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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Example of Example of multiwavelength multiwavelength campaign campaign

The OJ 287 campaign: some examples of radio data galore and multiwaveband SEDs.

Radio-to-X-ray spectral energy distribution (SED) of OJ 287 simultaneous to the 2 XMM-Newton

• bservations (OM and EPIC-pn data) of

Apr.12, and Nov.3-4, 2005. A synchrotron self-Compton (SSC) model for these 2 epochs is reported (red and blue continuous lines). OJ 287 from the LBL family, arisen to the IBL category, as during flaring phases it can emit synchrotron photons even at the soft X- ray band. (From Ciprini et al., in prep.). The radio-mm flux light curves of OJ 287 in different bands (frequencies span from 2.3 to 230 GHz),

• btained during the extended monitoring campaign,

and by independent observing programs. At a first inspection there is not a significant radio-optical correlation (From Ciprini et al. 2007, Ciprini et al., in prep.). 15GHz, 22GHz, 43GHz VLBA images and the map of the spectral index of the jet of OJ 287 obtained in April 2005. IDV ~ 3%

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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GLAST pre GLAST pre-

• launch MW proposals

launch MW proposals

3 dedicated MW proposals were also submitted before the launch of GLAST, as support and service for the GLAST coll., and for tentative GLAST MW campaigns (all the proposals were made on behalf of the GLAST coll.). All the 3 following proposals made as PI were not accepted (motivation: “GLAST is not flying”; “we would expect on-flight performances of GLAST” . …but “try again it Sam”, because now GLAST (and AGILE of course) are flying!

Spitzer Cycle-5 proposal: Investigating the far-mid infrared and gamma−ray connection in MeV (COMPTEL) blazars with Spitzer and GLAST. Observation of 7 MeV

• blazars. Comptonization of ambient infrared radiation from dust. Mid-far infrared

investigation of the dusty−stuffed ambient of flat spectrum radio quasars, where dust is produced and survive. Its relation with gamma-ray emission. XMM-Newton AO7 proposal: High-energy jet emission in intermediate blazars: the joined XMM-Newton and GLAST view. 3 bright intermediate-blazars (IBL), namely PKS 0735+178, GC 0109+224 (both IBL candidates with old X-rays analysis, and an interesting close environment) and W Com (the IBL prototype, with an observed twofold, synchrotron and inverse-Compton, X-ray spectrum). NOT P36 proposal: Optical polarimetric survey of new gamma-ray blazar candidates for

• GLAST. Optical polarimetric snapshots of a sample of relatively bright new blazar candidates,

selected by radio/optical X-rays surveys/catalogues.

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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11 observing seasons,

10 years light curves, 1637 photometric data points, almost 500 nights

• f observations.

Rapid optical variations connected to slower

• variations. Intermediate or

low level of activity. Long–term variability is essentially achromatic, whereas flares imply spectral changes. There is not clear hysteresis loops in the optical spectral index evolution during intermediate flares.

10 years (1994-2004) of optical monitoring data (BVRI bands) on PKS 0735+178 Data from

Perugia Univ. Obs. (the bulk of data), Torino Obs., Tuorla Obs., Sabadell

Example of long-term optical variability monitoring

Adapted from Ciprini et al. 2007

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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■ Discrete Correlation Function. ■ Structure Function SF. ■ Lomb-Scargle Periodogram. ■ Clean Discrete Fourier Transform.

Temporal behaviour: Temporal analysis of optical

• variability. To search for coherent time structures,

characteristic timescales, and to identify duty-cycles and variability modes . This is important for GLAST twice: 1) long-term and optical-gamma-rays correlation analysis; 2) standalone GLAST light curves analysis of bright gamma- ray blazars. GLAST will be able to observe variability on the same mid/long-term timescales monitored already in the

• ptical band!

Long-term (months-weeks); mid-term (days) timescales investigated.

Example of long-term optical variability monitoring

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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■ Phase Dispersion Minimization.

■ Gaps Window Function. periodogram GWFP. ■ Discrete Wavelet Transform scalogram*. Such methods can be applied to AGILE/GLAST long-term light curves

• f blazars.

Example of long-term optical variability monitoring

“AGILE 1st Year of Gamma-ray Astrophysics”, ESRIN, Frascati, Roma, 12-13 June 2008

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The end The end

Spectroscopy Polarization Variability Flux Monitoring Multiwaveband campaigns